The supernova-regulated ISM. I. The multi-phase structure

TL;DR

This paper presents detailed 3D simulations of the multi-phase interstellar medium influenced by supernovae, revealing a robust three-phase structure with specific density and temperature distributions, and analyzing flow scales and cooling effects.

Contribution

It introduces a comprehensive model of the supernova-regulated ISM, detailing the physical processes, phase classification, and statistical properties, with insights into the structure's robustness and flow scales.

Findings

Most of the ISM complexity is captured by three phases.

Gas density within each phase follows a lognormal distribution.

The flow correlation scale is about 100 pc, increasing with height.

Abstract

We simulate the multi-phase interstellar medium randomly heated and stirred by supernovae, with gravity, differential rotation and other parameters of the solar neighbourhood. Here we describe in detail both numerical and physical aspects of the model, including injection of thermal and kinetic energy by SN explosions, radiative cooling, photoelectric heating and various transport processes. With 3D domain extending 1 kpc^2 horizontally and 2 kpc vertically, the model routinely spans gas number densities 10^-5 - 10^2 cm^-3, temperatures 10-10^8 K, local velocities up to 10^3 km s^-1 (with Mach number up to 25). The thermal structure of the modelled ISM is classified by inspection of the joint probability density of the gas number density and temperature. We confirm that most of the complexity can be captured in terms of just three phases, separated by temperature borderlines at about 10^3 K and 5x10^5 K. The probability distribution of gas density within each phase is approximately lognormal. We clarify the connection between the fractional volume of a phase and its various proxies, and derive an exact relation between the fractional volume and the filling factors defined in terms of the volume and probabilistic averages. These results are discussed in both observational and computational contexts. The correlation scale of the random flows is calculated from the velocity autocorrelation function; it is of order 100 pc and tends to grow with distance from the mid-plane. We use two distinct parameterizations of radiative cooling to show that the multi-phase structure of the gas is robust, as it does not depend significantly on this choice.